Figure REF  shows a diffuse X-ray tail extending to the north at the center and that the cluster emission is elongated along northwest-southeast direction.
The hot gas emission (i) shows a compact, bright region and a diffuse tail extending to the north at the center, and (ii) is extended along the northwest–southeast direction showing pieces of evidence for surface-brightness edges. Though the X-ray peak emission and peak of the radio emission register well (see Figure REF , left), the position of the optical host of the southern cD galaxy (R.A.: 15:22:29.17, decl.: \(+\) 27:42:27.5) is displaced by \(\sim \) 24 from the compact, bright, X-ray peak emission at the cluster center (see Figure REF , right, and also Figure REF ). A low-surface-brightness diffuse tail, both in X-ray as well as in radio images, extending to the north at the center of the image, reaches out to the second cD galaxy (R.A.: 15:22:28.92, decl.: \(+\) 27:42:44.1; Figures REF  and REF , top-right panels). The X-ray peak corresponding to the second northern cD galaxy and the peak of the second weaker component of radio emission at this location also register well. The southern cD galaxy seems to have retained a cool core residing at the center of its subcluster and there is no evidence for a cool core corresponding to the northern cD galaxy [1]}, [2]}. The closely associated radio and X-ray morphology at the center and its connection with the southern cD galaxy suggest that both X-ray and radio emissions are due to ram pressure stripping as the southern cD galaxy moves relative to the ICM.
